Abstract
We present the detection of type C quasi-periodic oscillation (QPO) along with upper harmonic at respective frequencies of \(\sim \)0.6 Hz and \(\sim \)1.2 Hz in the single AstroSat observation taken during the 2016 outburst of the low-mass black hole X-ray binary H 1743-322. These frequencies are found to be shifted by \(\sim \)0.4 Hz for the QPO and \(\sim \)0.8 Hz for the upper harmonic with respect to that found in the simultaneous XMM-Newton and NuSTAR observation taken five days later than the AstroSat observation, indicating a certain geometrical change in the system. However, the centroid frequency of the QPO and the upper harmonic do not change with energy, indicating the energy-independent nature. The decreasing trend in the fractional rms of the QPO with energy is consistent with the previous results for this source in the low/hard state. The value of the photon index (\(\Gamma \sim 1.67\)) also indicates that the source was in the low/hard state during this particular observation. In addition, similar to the XMM-Newton observations during the same outburst, we find a hard lag of \(\sim \)21 ms in the frequency range of \(\sim \)1–5 Hz. The log-linear trend between the averaged time lag and energy indicates the propagation of fluctuations in the mass accretion rate from outer part of the accretion disk to the inner hot regions.
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Acknowledgements
We thank the anonymous referee for useful comments that have improved the quality of the paper. The authors acknowledge the financial support of ISRO under AstroSat archival Data utilization program (No: DS-2B-13013(2)/8/2019-Sec.2). This publication uses data from the AstroSat mission of the Indian Space Research Organisation (ISRO), archived at the Indian Space Science Data Centre (ISSDC). This work has used the data from SXT and LAXPC instruments onboard AstroSat. LAXPC data were processed by the Payload Operation Center (POC) at TIFR, Mumbai. This work has been performed utilizing the calibration data-bases and auxiliary analysis tools developed, maintained and distributed by the AstroSat-SXT team with members from various institutions in India and abroad, and the SXT POC at the TIFR, Mumbai (https://www.tifr.res.in/~astrosat_sxt/index.html). SXT data were processed and verified by the SXT POC. This research has also used the data from MAXI space telescope provided by RIKEN, JAXA and the MAXI team. VKA thanks GH, SAG; DD, PDMSA and Director, URSC for encouragement and continuous support to carry out this research. P.T. expresses his sincere thanks to the Inter-University Centre for Astronomy and Astrophysics (IUCAA), Pune, India, for granting supports through the IUCAA associateship program. S.C. is also very much grateful to IUCAA, Pune, India, for providing support and local hospitality during his frequent visits.
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This article is part of the Special Issue on "AstroSat: Five Years in Orbit".
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Chand, S., Agrawal, V.K., Dewangan, G.C. et al. AstroSat observation of 2016 outburst of H 1743-322. J Astrophys Astron 42, 38 (2021). https://doi.org/10.1007/s12036-020-09688-x
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DOI: https://doi.org/10.1007/s12036-020-09688-x